Context. Chemically inhomogeneous populations are observed in most globular clusters, but not in open clusters. Cluster mass seems to play a key role in the existence of multiple populations. Aims. Studying the chemical homogeneity of the most massive open clusters is needed to better understand the mechanism of their formation and determine the mass limit under which clusters cannot host multiple populations. Here we studied NGC 6705, which is a young and massive open cluster located towards the inner region of the Milky Way. This cluster is located inside the solar circle. This makes it an important tracer of the inner disk abundance gradient. Methods. This study makes use of BVI and ri photometry and comparisons with theoretical... (More)

Context. Chemically inhomogeneous populations are observed in most globular clusters, but not in open clusters. Cluster mass seems to play a key role in the existence of multiple populations. Aims. Studying the chemical homogeneity of the most massive open clusters is needed to better understand the mechanism of their formation and determine the mass limit under which clusters cannot host multiple populations. Here we studied NGC 6705, which is a young and massive open cluster located towards the inner region of the Milky Way. This cluster is located inside the solar circle. This makes it an important tracer of the inner disk abundance gradient. Methods. This study makes use of BVI and ri photometry and comparisons with theoretical isochrones to derive the age of NGC 6705. We study the density profile of the cluster and the mass function to infer the cluster mass. Based on abundances of the chemical elements distributed in the first internal data release of the Gaia-ESO Survey, we study elemental ratios and the chemical homogeneity of the red clump stars. Radial velocities enable us to study the rotation and internal kinematics of the cluster. Results. The estimated ages range from 250 to 316 Myr, depending on the adopted stellar model. Luminosity profiles and mass functions show strong signs of mass segregation. We derive the mass of the cluster from its luminosity function and from the kinematics, finding values between 3700 M-circle dot and 11 000 M-circle dot. After selecting the cluster members from their radial velocities, we obtain a metallicity of [Fe/H] = 0.10 +/- 0.06 based on 21 candidate members. Moreover, NGC 6705 shows no sign of the typical correlations or anti-correlations between Al, Mg, Si, and Na, which are expected in multiple populations. This is consistent with our cluster mass estimate, which is lower than the required mass limit proposed in the literature to develop multiple populations. (Less)

@article{00fbb7a5-71c4-40cf-b9ff-52cda4e9f509,
abstract = {Context. Chemically inhomogeneous populations are observed in most globular clusters, but not in open clusters. Cluster mass seems to play a key role in the existence of multiple populations. Aims. Studying the chemical homogeneity of the most massive open clusters is needed to better understand the mechanism of their formation and determine the mass limit under which clusters cannot host multiple populations. Here we studied NGC 6705, which is a young and massive open cluster located towards the inner region of the Milky Way. This cluster is located inside the solar circle. This makes it an important tracer of the inner disk abundance gradient. Methods. This study makes use of BVI and ri photometry and comparisons with theoretical isochrones to derive the age of NGC 6705. We study the density profile of the cluster and the mass function to infer the cluster mass. Based on abundances of the chemical elements distributed in the first internal data release of the Gaia-ESO Survey, we study elemental ratios and the chemical homogeneity of the red clump stars. Radial velocities enable us to study the rotation and internal kinematics of the cluster. Results. The estimated ages range from 250 to 316 Myr, depending on the adopted stellar model. Luminosity profiles and mass functions show strong signs of mass segregation. We derive the mass of the cluster from its luminosity function and from the kinematics, finding values between 3700 M-circle dot and 11 000 M-circle dot. After selecting the cluster members from their radial velocities, we obtain a metallicity of [Fe/H] = 0.10 +/- 0.06 based on 21 candidate members. Moreover, NGC 6705 shows no sign of the typical correlations or anti-correlations between Al, Mg, Si, and Na, which are expected in multiple populations. This is consistent with our cluster mass estimate, which is lower than the required mass limit proposed in the literature to develop multiple populations.},
articleno = {A17},
author = {Cantat-Gaudin, T. and Vallenari, A. and Zaggia, S. and Bragaglia, A. and Sordo, R. and Drew, J. E. and Eisloeffel, J. and Farnhill, H. J. and Gonzalez-Solares, E. and Greimel, R. and Irwin, M. J. and Kupcu-Yoldas, A. and Jordi, C. and Blomme, R. and Sampedro, L. and Costado, M. T. and Alfaro, E. and Smiljanic, R. and Magrini, L. and Donati, P. and Friel, E. D. and Jacobson, H. and Abbas, U. and Hatzidimitriou, D. and Spagna, A. and Vecchiato, A. and Balaguer-Nunez, L. and Lardo, C. and Tosi, M. and Pancino, E. and Klutsch, A. and Tautvaisiene, G. and Drazdauskas, A. and Puzeras, E. and Jimenez-Esteban, F. and Maiorca, E. and Geisler, D. and Roman, I. San and Villanova, S. and Gilmore, G. and Randich, S. and Bensby, Thomas and Flaccomio, E. and Lanzafame, A. and Recio-Blanco, A. and Damiani, F. and Hourihane, A. and Jofre, P. and de Laverny, P. and Masseron, T. and Morbidelli, L. and Prisinzano, L. and Sacco, G. G. and Sbordone, L. and Worley, C. C.},
issn = {0004-6361},
keyword = {stars: abundances,open clusters and associations: general,open,clusters and associations: individual: NGC 6705},
language = {eng},
publisher = {EDP Sciences},
series = {Astronomy & Astrophysics},
title = {The Gaia-ESO Survey: Stellar content and elemental abundances in the massive cluster NGC 6705},
url = {http://dx.doi.org/10.1051/0004-6361/201423851},
volume = {569},
year = {2014},
}